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\@writefile{lof}{\contentsline {figure}{\numberline {1}{\ignorespaces ACE at L1, between the Earth and the Sun.}}{1}}
\@writefile{lot}{\contentsline {table}{\numberline {1}{\ignorespaces ACE Instrumentation}}{2}}
\newlabel{table1}{{1}{2}}
\@writefile{lof}{\contentsline {figure}{\numberline {2}{\ignorespaces The ionic charge-state composition of Fe observed by SWICS/ACE during a CME in early May, 1998. Shown are 1-hour averages from two time periods; a movie that can be viewed at http://www.srl.caltech.edu/ACE/ACENews16.html shows the entire time history of this event.}}{3}}
\@writefile{lof}{\contentsline {figure}{\numberline {3}{\ignorespaces The intensity of oxygen nuclei from $\sim 0.06$ to $\sim 50$ MeV/nuc observed by the ULEIS and SIS instruments on ACE during the large SEP events of early November, 1997.}}{3}}
\@writefile{lof}{\contentsline {figure}{\numberline {4}{\ignorespaces Variation in the ionic charge state composition of oxygen observed by SEPICA/ACE during the Nov. 6, 1997 solar particle event. A rough estimate yields a temperature of $\sim 2 \times 10^6$ for the first period and $\sim 2.3 \times 10^6$ K for the second.}}{4}}
\@writefile{lof}{\contentsline {figure}{\numberline {5}{\ignorespaces Quiet-time energy spectra of O and Ne isotopes observed by SIS/ACE showing anomalous cosmic ray enhancements in the rare isotopes $^{18}$O and $^{22}$Ne.}}{4}}
\@writefile{lof}{\contentsline {figure}{\numberline {6}{\ignorespaces The top two panels show mass histograms of cobalt and nickel isotopes observed by CRIS. Note the low abundance of $^{59}$Ni. The curves show calculations of how the abundances of $^{59}$Ni and $^{59}$Co are expected to depend on the elapsed time between the supernova explosion and cosmic ray acceleration. The hatched bands show ranges of $^{59}$Ni and $^{59}$Co that are consistent with the data, indicating a time delay of $>10^5$ years.}}{5}}